Proposal 13811 (STScI Edit Number: 0, Created: Friday, July 18, 2014 8:11:28 PM EST) - Overview
13811 - Feedback in action in the type 1 Seyfert IZw 1
Cycle: 22, Proposal Category: GO
(Availability Mode: SUPPORTED)
INVESTIGATORS
Name
Dr. Elisa Costantini (PI) (ESA Member) (Contac
t)
Dr. Luigi Gallo (CoI)
Dr. W. Nielsen Brandt (CoI)
Prof. Andrew C. Fabian (CoI) (ESA Member)
Dr. Gerard A. Kriss (CoI) (Contact)
Dr. Catia Silva (CoI) (ESA Member)
Dr. Laura di Gesu (CoI) (ESA Member)
VISITS
Visit Targets used in Visit
Institution
Space Research Organization Netherlands
E-Mail
e.costantini@sron.nl
Saint Mary's University
The Pennsylvania State University
University of Cambridge
Space Telescope Science Institute
Space Research Organization Netherlands
Space Research Organization Netherlands
lgallo@ap.smu.ca
niel@astro.psu.edu
acf@ast.cam.ac.uk
gak@stsci.edu
c.silva@sron.nl
l.di.gesu@sron.nl
Configurations used in Visit
Orbits Used Last Orbit Planner Run
01
(1) IZW1
COS/FUV
COS/NUV
4
18-Jul-2014 21:11:23.0
OP Current
with Visit?
yes
02
(1) IZW1
COS/FUV
COS/NUV
4
18-Jul-2014 21:11:26.0
yes
8 Total Orbits Used
ABSTRACT
We propose simultaneous 200 ks XMM-Newton-RGS and HST-COS observations of the narrow line Seyfert1 IZw1. We will study the connection
between the X-ray and UV absorber, mapping the ionization structure, kinematic behavior and elemental abundances. Finally we will quantify the
1
Proposal 13811 (STScI Edit Number: 0, Created: Friday, July 18, 2014 8:11:28 PM EST) - Overview
AGN feedback by directly measuring the metal enrichment by C, N, O, and Fe and the kinetic luminosity of the outflow.
OBSERVING DESCRIPTION
We will observe I Zw1 with HST-COS for 8 orbits organized into 2 identical visits. Both visits should be within days of each other, and coordinated
with an approved XMM-Newton observation of I Zw 1. This will allow us to study the combined UV-X-ray properties of the outflowing gas, not not
only in the strong Ly alpha and CIV troughs, but also among others such as N V (1238,1242 A) and Si IV(1393,1402 A) transitions. A large number
of ions will put more stringent constraints on the ionization parameter of the multi-kinetic components of the UV gas. The sensitivity of COS will
also allow us to study metastable levels such as CIII* at =1176 A. These excited levels have a similar ionization of the UVX-ray absorbers and
provide valuable density (and therefore distance) diagnostic measurements. We will reanalyze the FUSE data with updated methods for an estimate
of the CIII ground level transition (977 A). Even a non-detection of CIII will put useful upper limit on the gas density.
I Zw1 has been recently observed (Nov 2012) using the G130M grating of COS for a total of only 1.8 ks. A preliminary look at the data highlights
the broad Ly alpha trough, outflowing at 2000 km s^{-1}, tentatively confirming the existence of the long-lived UV-X-ray outflow, which possibly
varies only in ionization state. CIII* 1176 is tentatively identified, possibly outflowing, but the
present quality of the data makes it difficult to disentagle it from other intrinsic and Galactic lines. We will therefore observe I Zw 1 using both the
G130M grating for ~6 ks and the G160M grating for ~11 ks in order to reach a S/N of 20 in the continuum. This will assure a S/N=10 in the bottom
of the UV absorption troughs, which will enable us to determine the covering fraction of the absorbing gas to an accuracy of 10%. The enhanced
exposure time for G160M relative to G130M is needed to compensate for its lower sensitivity. We based our ETC calculations using the fluxes
of the COS data already acquired, considering a flux of 1e-14 erg cm^{-2} s^{-1} A^{-1} at 1440 A.
We use multiple central wavelength settings and multiple FP-POS positions to bridge the gap between detector segments, and to avoid detector and
flat-field artifacts. Central wavelengths and FP-POS positiopns were chosen to avoid placing the gap in wavelength regions corresponding to features
of interest, as described in our comments for each exposure.
To allow for source variability, we have chosen BUFFER TIMES significantly shorter than the 2/3 factor recommended in the ETC. We have also
chosen the BUFFER TIMES to be integer multiples of (exposure time - 110 s) to minimze the overheads due to buffer readouts between successive
exspoures.
2
Proposal 13811 (STScI Edit Number: 0, Created: Friday, July 18, 2014 8:11:28 PM EST) - Overview
These observations pose no bright object concerns. All historical flux levels for I Zw 1 lie below the bright object limits for COS (see Dunn et al.
2006, PASP, 118, 572). Since I Zw 1 has been observed successfully before, there are also no surrounding field objects that are too bright. This is
confirmed by the BOT tool for GALEX in APT.
3
Fixed Targets Diagnostics
Visit
Proposal 13811 - Visit 01 - Feedback in action in the type 1 Seyfert IZw 1
Proposal 13811, Visit 01
Diagnostic Status: Warning
Scientific Instruments: COS/NUV, COS/FUV
Special Requirements: SCHED 100%
Comments: Visit 1 should be scheduled within days of Visit 2. Both should be coordinated with approved XMM-Newton observations of I Zw 1.
(Visit 01) Warning (Form): For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
#
(1)
Name
IZW1
Target Coordinates
RA: 00 53 34.9300 (13.3955417d)
Dec: +12 41 36.19 (12.69339d)
Equinox: J2000
Targ. Coord. Corrections
Redshift: 0.0589
4
Fluxes
V=14.1+/-0.1
1.0e-14 at 1440 A
Sat Jul 19 01:11:28 GMT 2014
Miscellaneous
Reference Frame: ICRS
Proposal 13811 - Visit 01 - Feedback in action in the type 1 Seyfert IZw 1
#
1
Label
Target
(ETC Run)
(COS.ta.618 (1) IZW1
535)
Config,Mode,Aperture
Spectral Els.
COS/NUV, ACQ/IMAGE, PSA
MIRRORB
Opt. Params.
Groups
Exp. Time (Total)/[Actual Dur.]
100 Secs (100 Secs)
[==>]
Comments: Exposure time increased by 4x from ETC to allow for source variability.
2
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G130M
529)
1291 A
Exposures
Special Reqs.
BUFFER-TIME=42
960 Secs (960 Secs)
5;
[==>]
FP-POS=4
Comments: FP-POS=4 gives shortest wavelengths for G130M/1289. But, B->A segment gap onpeak of redshifted Ly alpha, so only want one exposure here.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
3
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G130M
BUFFER-TIME=42
950 Secs (950 Secs)
529)
0;
1327 A
[==>]
FP-POS=4
Comments: FP-POS=1 for 1327 puts the gap from in the red wing of redshifted N V.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
4
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G130M
BUFFER-TIME=42
950 Secs (950 Secs)
529)
0;
1309 A
[==>]
FP-POS=3
Comments: FP-POS=3 and 4 puts the B->A segment gap in the red wing of redshifted Ly alpha, and well blueshifted from N V. Avoids the gaps from 1291 and 1327.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
5
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G130M
BUFFER-TIME=42
950 Secs (950 Secs)
529)
0;
1309 A
[==>]
FP-POS=4
Comments: FP-POS=3 and 4 puts the B->A segment gap in the red wing of redshifted Ly alpha, and well blueshifted from N V. Avoids the gaps from 1291 and 1327.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
6
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G160M
BUFFER-TIME=33
440 Secs (440 Secs)
675)
0;
1577 A
[==>]
FP-POS=1
Comments: 1577 and 1589 place the gap far in the blue wing of redshifted C IV, so concentrate exposures on FP-POS in each that bridge the gap between the segments.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
7
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G160M
BUFFER-TIME=39
1280 Secs (1280 Secs)
675)
0;
1577 A
[==>]
FP-POS=2
Comments: 1577 and 1589 place the gap far in the blue wing of redshifted C IV, so concentrate exposures on FP-POS in each that bridge the gap between the segments.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
8
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G160M
BUFFER-TIME=39
1280 Secs (1280 Secs)
675)
0;
1577 A
[==>]
FP-POS=3
Comments: 1577 and 1589 place the gap far in the blue wing of redshifted C IV, so concentrate exposures on FP-POS in each that bridge the gap between the segments.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
9
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G160M
BUFFER-TIME=39
1280 Secs (1280 Secs)
675)
0;
1589 A
[==>]
FP-POS=3
Comments: 1577 and 1589 place the gap far in the blue wing of redshifted C IV, so concentrate exposures on FP-POS in each that bridge the gap between the segments.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
5
Orbit
[1]
[1]
[1]
[2]
[2]
[2]
[3]
[3]
[4]
Proposal 13811 - Visit 01 - Feedback in action in the type 1 Seyfert IZw 1
10
(COS.sp.618 (1) IZW1
675)
COS/FUV, TIME-TAG, PSA
G160M
1589 A
BUFFER-TIME=39
1280 Secs (1280 Secs)
0;
[==>]
FP-POS=4
Comments: 1577 and 1589 place the gap far in the blue wing of redshifted C IV, so concentrate exposures on FP-POS in each that bridge the gap between the segments.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
6
[4]
Orbit Structure
Proposal 13811 - Visit 01 - Feedback in action in the type 1 Seyfert IZw 1
7
Proposal 13811 - Visit 01 - Feedback in action in the type 1 Seyfert IZw 1
8
Fixed Targets Diagnostics
Visit
Proposal 13811 - Visit 02 - Feedback in action in the type 1 Seyfert IZw 1
Proposal 13811, Visit 02
Diagnostic Status: Warning
Scientific Instruments: COS/NUV, COS/FUV
Special Requirements: SCHED 100%
Comments: Visit 2 should be scheduled within days of Visit 1. Both should be coordinated with approved XMM-Newton observations of I Zw 1.
(Visit 02) Warning (Form): For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
#
(1)
Name
IZW1
Target Coordinates
RA: 00 53 34.9300 (13.3955417d)
Dec: +12 41 36.19 (12.69339d)
Equinox: J2000
Targ. Coord. Corrections
Redshift: 0.0589
9
Fluxes
V=14.1+/-0.1
1.0e-14 at 1440 A
Sat Jul 19 01:11:29 GMT 2014
Miscellaneous
Reference Frame: ICRS
Proposal 13811 - Visit 02 - Feedback in action in the type 1 Seyfert IZw 1
#
1
Label
Target
(ETC Run)
(COS.ta.618 (1) IZW1
535)
Config,Mode,Aperture
Spectral Els.
COS/NUV, ACQ/IMAGE, PSA
MIRRORB
Opt. Params.
Groups
Exp. Time (Total)/[Actual Dur.]
100 Secs (100 Secs)
[==>]
Comments: Exposure time increased by 4x from ETC to allow for source variability.
2
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G130M
529)
1291 A
Exposures
Special Reqs.
BUFFER-TIME=42
960 Secs (960 Secs)
5;
[==>]
FP-POS=4
Comments: FP-POS=4 gives shortest wavelengths for G130M/1289. But, B->A segment gap onpeak of redshifted Ly alpha, so only want one exposure here.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
3
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G130M
BUFFER-TIME=42
950 Secs (950 Secs)
529)
0;
1327 A
[==>]
FP-POS=4
Comments: FP-POS=1 for 1327 puts the gap from in the red wing of redshifted N V.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
4
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G130M
BUFFER-TIME=42
950 Secs (950 Secs)
529)
0;
1309 A
[==>]
FP-POS=3
Comments: FP-POS=3 and 4 puts the B->A segment gap in the red wing of redshifted Ly alpha, and well blueshifted from N V. Avoids the gaps from 1291 and 1327.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
5
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G130M
BUFFER-TIME=42
950 Secs (950 Secs)
529)
0;
1309 A
[==>]
FP-POS=4
Comments: FP-POS=3 and 4 puts the B->A segment gap in the red wing of redshifted Ly alpha, and well blueshifted from N V. Avoids the gaps from 1291 and 1327.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
6
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G160M
BUFFER-TIME=33
440 Secs (440 Secs)
675)
0;
1577 A
[==>]
FP-POS=1
Comments: 1577 and 1589 place the gap far in the blue wing of redshifted C IV, so concentrate exposures on FP-POS in each that bridge the gap between the segments.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
7
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G160M
BUFFER-TIME=39
1280 Secs (1280 Secs)
675)
0;
1577 A
[==>]
FP-POS=2
Comments: 1577 and 1589 place the gap far in the blue wing of redshifted C IV, so concentrate exposures on FP-POS in each that bridge the gap between the segments.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
8
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G160M
BUFFER-TIME=39
1280 Secs (1280 Secs)
675)
0;
1577 A
[==>]
FP-POS=3
Comments: 1577 and 1589 place the gap far in the blue wing of redshifted C IV, so concentrate exposures on FP-POS in each that bridge the gap between the segments.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
9
(COS.sp.618 (1) IZW1
COS/FUV, TIME-TAG, PSA
G160M
BUFFER-TIME=39
1280 Secs (1280 Secs)
675)
0;
1589 A
[==>]
FP-POS=3
Comments: 1577 and 1589 place the gap far in the blue wing of redshifted C IV, so concentrate exposures on FP-POS in each that bridge the gap between the segments.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
10
Orbit
[1]
[1]
[1]
[2]
[2]
[2]
[3]
[3]
[4]
Proposal 13811 - Visit 02 - Feedback in action in the type 1 Seyfert IZw 1
10
(COS.sp.618 (1) IZW1
675)
COS/FUV, TIME-TAG, PSA
G160M
1589 A
BUFFER-TIME=39
1280 Secs (1280 Secs)
0;
[==>]
FP-POS=4
Comments: 1577 and 1589 place the gap far in the blue wing of redshifted C IV, so concentrate exposures on FP-POS in each that bridge the gap between the segments.
Buffer time reduced by more than 2/3 of the ETC value to allow for source variability.
Buffer times also chosen to be (exposure time - 110 s)/n to minimize overheads due to buffer dumps between exposures.
11
[4]
Orbit Structure
Proposal 13811 - Visit 02 - Feedback in action in the type 1 Seyfert IZw 1
12
Proposal 13811 - Visit 02 - Feedback in action in the type 1 Seyfert IZw 1
13